We present the results of a ~160 ks-long XMM-Newton observation of the Seyfert 1 galaxy Mrk 279.
The spectrum shows evidence of both broad and narrow emission features. The Fe Kα line may be equally well explained by a
single broad Gaussian (FWHM ~ 10 000 km s-1) or by two components: an unresolved core plus a very broad profile
(FWHM ~ 14 000 km s-1). For the first time we quantified, via the “locally
optimally emitting cloud” model, the contribution of the broad line region (BLR) to the absolute luminosity of
the broad component of the Fe Kα at 6.4 keV.
We find that the contribution of the BLR is only ~3%.
In the two-line component scenario, we also evaluated
the contribution of the highly ionized gas component, which produces the Fe xxvi line in the iron K region. This
contribution to the narrow core of the Fe Kα line is marginal <0.1%. Most of the
luminosity of the unresolved, component of Fe Kα may come from the obscuring torus,
while the very-broad associated
component may come from the accretion disk. However, models of reflection by cold gas are difficult to test because
of the limited energy band. The Fe xxvi line at 6.9 keV is consistent to be produced
in a high column density (NH ~ 1023 cm-2), extremely ionized (log ξ ~ ) gas.
This gas may be a highly
ionized outer layer of the torus.

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